Interstellar dust plays a critical role in galaxy assembly. Dust grains are a site of efficient molecule formation, specifically H\(_2\) , the fuel for new star formation (e.g., [1]}). Dust grains also affect how we observe galaxy assembly: the cosmic infrared background is equivalent in power to the cosmic optical background (e.g., [2]}), implying that about half of all the UV/optical light produced by stars in the Universe is reprocessed by dust. In fact, we know that dust-obscured star formation contributes significantly to the total star formation rate (SFR) density of the Universe (e.g., [3]}). Recent studies show that dust-obscured star formation dominates the cosmic SFR density out to at least \(z\simeq 3\)  (e.g., [4]}), and it still provides an important contribution at higher redshifts, although the exact amount of dust-obscured star formation at the earliest redshifts (\(z\gtrsim 6\) , i.e., in the epoch of reionization, or `cosmic dawn') is still uncertain.
